Sediment transport by liquid surficial flow: Application to Titan     

Devon M. Burr  Joshua P. Emery  Geoffrey C. Collins 《Icarus》2006,181(1):235-242

Sediment transport by surficial flow likely occurs on Titan. Titan is thought to have a volatile cycle, such as on Earth and likely in the past on Mars, which would entail surficial liquid flow. And surficial flow is implied in interpretations of Cassini-Hyugens data as showing fluvial channels, which would require sediment transport by surficial flow to form the observable features. We present calculations from basic hydraulic formulae of sediment entrainment and transport by surficial flow. First, we describe the conditions for (non-cohesive) sediment entrainment by grain size through use of the Shields' threshold curve. We then calculate settling velocities by grain size to describe the type of sediment transport—washload, suspended load, or bedload—that would follow entrainment. These calculations allow derivation of required flow depths for sediment transport by grain size over a given slope. A technique to estimate required flow velocities and unit discharges is also presented. We show the results of these calculations for organic and water ice sediment movement by liquid methane flow under Titan gravity. For comparative purposes, plots for movement of quartz sediment by water on Earth and basalt sediment by water on Mars are also included. These results indicate that (non-cohesive) material would move more easily on Titan than on Earth or Mars. Terrestrial field observations suggest that coarse grain transport is enhanced by hyperconcentration of fine-grained sediment; and the apparent availability of organic (fine grained) sediment on Titan, in conjunction with the possibility of convection-driven rainstorms, may lead to hyperconcentrated flows. Thus, significant sediment transport may occur on Titan during individual overland flow events.  相似文献   

Multiple emission angle surface-atmosphere separations of thermal emission spectrometer data     

Joshua L Bandfield  Michael D Smith 《Icarus》2003,161(1):47-65

A method for separating the spectral signatures of the Martian surface and atmosphere was developed and is applied to multiple emission angle data returned from the MGS TES instrument. This method includes correlated-k and index gas removal algorithms that may be applied to all nadir-pointing TES data. Initial results have provided new and refined measurements of the spectral shapes of atmospheric dust and the Martian surface. Surface temperatures and atmospheric dust opacities are also retrieved with improved accuracy over single observation temperature and opacity retrievals. Low-albedo surfaces display absorptions consistent in both shape and depth with previous studies. These surfaces may be closely modeled using a combination of previously derived basalt, andesitic, and high-albedo surface spectral shapes. Short wavelengths display no significant absorptions, indicating both the coarse particulate nature of the surface and the lack of significant amounts of carbonate. Moderate- and high-albedo surfaces have spectral shapes distinctive of fine particulate silicate materials. No single material can match the entire high-albedo surface spectrum, though there are clear indications of a material that closely matches intermediate to calcic plagioclase and an emission peak at ∼1620 cm⁻¹ due to bound water. The lack of residual restrahlen silicate absorptions indicates that minerals such as olivine or pyroxene are not present in high-albedo surfaces at significant (but unknown) abundances. High-albedo surface results presented here are in agreement with and complementary to shorter wavelength observations. The Martian dust is composed of both primary and secondary minerals. Either chemical weathering has not completely altered its source material or the soil is a mixture of altered and unaltered sources. Further laboratory studies are needed to better establish detection limits and behavior of mineral mixtures of fine particulates in the thermal infrared portion of the spectrum.  相似文献   

Looking beyond the fisheries crisis: Cumulative learning from small-scale fisheries through diagnostic approaches     

Joshua E. Cinner  M. Aaron MacNeil  Xavier Basurto  Stefan Gelcich 《Global Environmental Change》2013,23(6):1359-1365

The common scientific and media narrative in fisheries is one of failure: poor governance, collapsed stocks, and vanishing livelihoods. Yet, there are successful fisheries – instances where governments and/or communities have maintained or rebuilt stocks, where fishers have robust livelihoods, and where institutions are strong. Scientists and managers alike are becoming increasingly interested in moving beyond the doom-and-gloom stories of fisheries failures toward cumulative knowledge for making fisheries governance more successful. Recent literature has attempted to determine what separates the successes from the failures and better understand how lessons learned for effective fisheries governance can be cumulatively compiled. In this special issue, we present a range of fisheries studies from around the world – Latin America, The Pacific, and East Africa. The studies look at varying fisheries outcomes, including sustainability, cooperation, self-governance, and sustaining livelihoods. The contributions in this special issue all tackle the challenge of exploring, testing, and refining the Diagnostic Framework for Analyzing Social-Ecological Systems developed by Elinor Ostrom as a way to cumulate knowledge on the potential conditions that could be causing a problem or creating a benefit in the governance of small-scale marine fisheries. These articles successfully explore the applicability and contributions of the framework while providing important theoretical refinements for small-scale fisheries.  相似文献   

Outer Main Belt asteroids: Identification and distribution of four 3-μm spectral groups     

Driss Takir  Joshua P. Emery 《Icarus》2012,219(2):641-654

This paper examines the distribution and the abundance of hydrated minerals (any mineral that contains H₂O or OH) on outer Main Belt asteroids spanning the 2.5 < a < 4.0 AU region. The hypothesis we are testing is whether planetesimals that accreted closer to the Sun experienced a higher degree of aqueous alteration. We would expect then to see a gradual decline of the abundance of hydrated minerals among the outer Main Belt asteroids with increasing heliocentric distance (2.5 < a < 4.0 AU). We measured spectra (0.8–2.5 μm and 1.9–4.1 μm) of 28 outer Main Belt asteroids using the SpeX spectrograph/imager at the NASA Infrared Telescope Facility (IRTF). We identified four groups on the basis of the shape and the band center of the 3-μm feature. The first group, which we call “sharp”, exhibits a sharp 3-μm feature, attributed to hydrated minerals (phyllosilicates). Most asteroids in this group are located in the 2.5 < a < 3.3 AU region. The second group, which we call “Ceres-like”, consists of 10 Hygiea and 324 Bamberga. Like Asteroid Ceres, these asteroids exhibit a 3-μm feature with a band center of 3.05 ± 0.01 μm that is superimposed on a broader absorption feature from ～2.8 to 3.7 μm. The third group, which we call “Europa-like”, includes 52 Europa, 31 Euphrosyne, and 451 Patientia. Objects in this group exhibit a 3-μm feature with a band center of 3.15 ± 0.01 μm. Both the Ceres-like and Europa-like groups are concentrated in the 2.5 < a < 3.3 AU region. The fourth group, which we call “rounded”, is concentrated in the 3.4 < a < 4.0 AU region. Asteroids in this group are characterized by a rounded 3-μm feature, attributed to H₂O ice. A similar rounded 3-μm feature was also identified in 24 Themis and 65 Cybele. Unlike the sharp group, the rounded group did not experience aqueous alteration. Of the asteroids observed in this study, 140 Siwa, a P-type, is the only one that does not exhibit a 3-μm feature. These results are important to constrain the nature and the degree of aqueous alteration in outer Main Belt asteroids.  相似文献   

A late Quaternary paleotemperature record from Hanging Lake, northern Yukon Territory, eastern Beringia     

Joshua Kurek  Les C. Cwynar  Jesse C. Vermaire   《Quaternary Research》2009,72(2):246-257

The late Quaternary paleoclimate of eastern Beringia has primarily been studied by drawing qualitative inferences from vegetation shifts. To quantitatively reconstruct summer temperatures, we analyzed lake sediments for fossil chironomids, and additionally we analyzed the sediments for fossil pollen and organic carbon content. A comparison with the δ¹⁸O record from Greenland indicates that the general climatic development of the region throughout the last glaciation–Holocene transition differed from that of the North Atlantic region. Between  17 and 15 ka, mean July air temperature was on average 5°C colder than modern, albeit a period of near-modern temperature at  16.5 ka. Total pollen accumulation rates ranged between  180 and 1200 grains cm^− 2 yr^− 1. At  15 ka, approximately coeval with the Bølling interstadial, temperatures again reached modern values. At  14 ka, nearly 1000 yr after warming began, Betula pollen percentages increased substantially and mark the transition to shrub-dominated pollen contributors. Chironomid-based inferences suggest no evidence of the Younger Dryas stade and only subtle evidence of an early Holocene thermal maximum, as temperatures from  15 ka to the late Holocene were relatively stable. The most recognizable climatic oscillation of the Holocene occurred from  4.5 to 2 ka.  相似文献   

Estimating the redshift distribution of photometric galaxy samples – II. Applications and tests of a new method     

Carlos E. Cunha  Marcos Lima  Hiroaki Oyaizu  Joshua Frieman  Huan Lin 《Monthly notices of the Royal Astronomical Society》2009,396(4):2379-2398

In Lima et al. we presented a new method for estimating the redshift distribution,   N ( z )  , of a photometric galaxy sample, using photometric observables and weighted sampling from a spectroscopic subsample of the data. In this paper, we extend this method and explore various applications of it, using both simulations and real data from the Sloan Digital Sky Survey (SDSS). In addition to estimating the redshift distribution for an entire sample, the weighting method enables accurate estimates of the redshift probability distribution,   p ( z )  , for each galaxy in a photometric sample. Use of   p ( z )  in cosmological analyses can substantially reduce biases associated with traditional photometric redshifts, in which a single redshift estimate is associated with each galaxy. The weighting procedure also naturally indicates which galaxies in the photometric sample are expected to have accurate redshift estimates, namely those that lie in regions of photometric-observable space that are well sampled by the spectroscopic subsample. In addition to providing a method that has some advantages over standard photo- z estimates, the weights method can also be used in conjunction with photo- z estimates e.g. by providing improved estimation of   N ( z )  via deconvolution of   N ( z _phot)  and improved estimates of photo- z scatter and bias. We present a publicly available   p ( z )  catalogue for ∼78 million SDSS DR7 galaxies.  相似文献   

A peculiar H i cloud near the distant globular cluster Pal 4     

Jacco Th. van Loon  Sne&#;ana Stanimirovi&#;  Mary E. Putman  Joshua E. G. Peek  Steven J. Gibson  Kevin A. Douglas  Eric J. Korpela 《Monthly notices of the Royal Astronomical Society》2009,396(2):1096-1105

We present 21-cm observations of four Galactic globular clusters, as part of the on-going Galactic Arecibo L-band Feed Array (GALFA) H  i survey at Arecibo. We discovered a peculiar H  i cloud in the vicinity of the distant (109 kpc) cluster Pal 4, and discuss its properties and likelihood of association with the cluster. We conclude that an association of the H  i cloud and Pal 4 is possible, but that a chance coincidence between Pal 4 and a nearby compact high-velocity cloud cannot be ruled out altogether. New, more stringent upper limits were derived for the other three clusters: M 3, NGC 5466, and Pal 13. We briefly discuss the fate of globular cluster gas and the interaction of compact clouds with the Galactic halo gas.  相似文献   

Hydrodynamical and radiative transfer modeling of meteoroid impacts into Saturn's rings     

Lindsey S. Chambers  Jeffrey N. Cuzzi  Joshua Colwell 《Icarus》2008,194(2):623-635

In a small hypervelocity impact, superheated gas and particles glow brightly with thermal emission for a brief time interval at short wavelengths; this phenomenon is referred to as an impact flash. Over the past decade, impact flashes have been observed on the Moon and in the laboratory in both the IR and visible portions of the spectrum. These phenomena have been used to constrain impactor parameters, such as impact size, velocity and composition. With the arrival of the Cassini spacecraft at Saturn, we embarked on a study of impact flashes in Saturn's rings. We present results on the feasibility of observing impact flashes and therefore estimating the flux of meteoroids impacting Saturn's rings using Cassini's Ultraviolet Imaging Spectrograph (UVIS). Our modeling effort is two-fold. We start by simulating impacts using the CTH hydrodynamical code. Impacts involve an icy ring particle and a serpentine meteoroid, modeled with the ANEOS equation of state. The objects are centimeters to meters in diameter and collide at 30 to 50 km s⁻¹. We then use the resulting temperatures and densities of the impact plumes in a radiative transfer calculation. We calculate bound-free, free-free, electron scattering and negative ion opacities along a line-of-sight through the center of each impact plume. Our model has shown that impact flashes will not be seen with the UVIS because (1) the plumes are optically thick when their central temperatures are high, with photosphere temperatures too cool to emit observable UV flux and (2) when the plumes become optically thin, even the hottest region of the plume is too cool to observe in the UV. This corroborates the lack of UVIS impact flash detections to date. Impact flashes are not likely to be seen by other Cassini instruments because of the short lifetimes of the plumes.  相似文献   

Impact of seawater temperature on growth and recruitment of invasive fouling species at the global scale          下载免费PDF全文

Joshua P. Lord 《Marine Ecology》2017,38(2)

Epibenthic fouling communities are dominated by invasive species that are globally distributed and can have substantial ecological and economic impacts in coastal habitats. Little is known about inter‐specific differences in life history strategies that cosmopolitan invasive species employ to acquire space and succeed in invaded habitats. The goal of this study was to examine the impact of seawater temperature on recruitment and growth of several cosmopolitan fouling species including the tunicates Botrylloides violaceus, Botryllus schlosseri and Diplosoma listerianum, as well as the bryozoans Bugula neritina and Watersipora subtorquata. To do this, the iBARGE (Invasive Bryozoan and Ascidian Recruitment and Growth Experiment) program was developed, utilizing a global network of collaborators to examine patterns over a broad geographic scale and a wide range of naturally varying seawater temperatures. This project produced a data set of thousands of photographs from 18 marinas in five countries in summer 2014 and 2015, allowing for recruitment and growth to be tabulated at a variety of temperatures. Thermal growth curves were established for five invasive species, and growth was compared among temperatures across sites, revealing a significant thermal effect. Recruitment was linked to temperature, with generally higher recruitment at warmer seawater temperatures and the highest peak recruitment values for the bryozoan Bugula neritina. Temperature also changed the relative importance of growth and recruitment for several species. These results paint a complex picture of the interactions among invasive fouling species as they relate to seawater temperature.  相似文献   

Racialized places, racialized bodies: the impact of racialization on individual and place identities     

Joshua F. Inwood  Robert A. Yarbrough 《GeoJournal》2010,75(3):299-301

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